Stability and observational properties of strange dwarfs

Yu.L. Vartanyan, G.S. Hajyan, A.K. Grigoryan and T.P. Sarkisyan1


We study the stability of strange dwarfs, i.e., superdense stars with small quark cores (Mcore/Modot < 0.017) and extended crusts consisting of atomic nuclei and degenerate electron gas, where the density can be greater by two orders of magnitude than the maximum density of white dwarfs. The mass, total number of baryons and radii of such configurations are unambiguously determined by the central energy density rc and the crust energy density rtr over the surface of the quark core. Using a static criterion, we define the state of stability loss for strange dwarfs in the whole range of rc and rtr. It has been shown that the gravitational redshifts of white and strange dwarfs are significantly distinguishable in the ranges of small and large (limiting) masses.


  1. N. K. Glendenning, Ch. Kettner, F. Weber, Phys. Rev.L 74 3519 (1995).
  2. N. K. Glendenning, Ch. Kettner, and F. Weber, Astrophys. J. 450, 253 (1995).
  3. Yu. L. Vartanian, A. K. Grigorian, and T. Sarkissian, Astrofizika 47, 223 (2004).
  4. C. Alcock, E. Farhi, and A. Olinto, Astrophys. J. 310, 261 (1986).
  5. R. C. Tolman, Phys. Rev. 55, 354 (1939).
  6. J. R. Oppenheimer and G. M. Volkoff, Phys. Rev. 55, 374 (1939).
  7. S. Chandrasekhar, Phys. Rev.L 12 114 (1964); Astrophys. J. 140, 417 (1964).
  8. Ya. B. Zel'dovich, Voprosy Kosmogonii 9, 157 (1963) (USSR Acad. Sci. Publishers).
  9. A. Chodos, R. L. Jaffe, K. Johnson, C. B. Thorne, and V. F. Wiesskopf, Phys. Rev. D 9, 3471 (1971).
  10. G. Baym, C. Pethick, and P. Sutherland, Astrophys. J. 170, 299 (1971).
  11. R. P. Feynman, N. Metropolis, and E. Teller, Phys. Rev. 75, 469 (2001).
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